ALMA CO and VLT/SINFONI H2 observations of the Antennae overlap region: mass and energy dissipation

TL;DR

This study uses ALMA and VLT/SINFONI observations to analyze molecular complexes in the Antennae galaxy merger, revealing their kinematics, energy dissipation processes, and potential early stages of super-star cluster formation.

Contribution

It provides new insights into the velocity structure, shock-driven H2 emission, and energy dissipation in super-giant molecular complexes during galaxy mergers.

Findings

H2 and CO kinematics are well matched in SGMCs.

H2/CO line ratios vary significantly among complexes.

A potential pre-cluster cloud with high H2/CO ratio was identified.

Abstract

We present an analysis of super-giant molecular complexes (SGMCs) in the overlap region of the Antennae galaxy merger, based on ALMA CO(3-2) interferometry and VLT/SINFONI imaging spectroscopy of H2 1-0 S(1) at angular resolutions of 0.9" and 0.7", respectively. All but one SGMC have multiple velocity components offset from each other by up to 150 km/s. H2 line emission is found in all SGMCs and the kinematics of H2 and CO are well matched. H2/CO line ratios vary by up to a factor of 10 among SGMCs and different velocity components of the same SGMCs. We also identify the CO counterpart of a bright, compact source of near-IR H2 line emission, which shows no Brgamma, and was first identified with SINFONI. This source has the highest H2/CO line ratio, and coincides with the steepest CO velocity gradient of the entire overlap region. With a size of 50 pc and a virial mass of a few 10^7 Msun it is perhaps a pre-cluster cloud that has not yet formed significant numbers of massive stars. We present observational evidence that the H2 emission is powered by shocks, and demonstrate how the H2 1-0 S(1) and the CO(3-2) lines can be used as tracers of energy dissipation and gas mass, respectively. The variations in the H2/CO line ratio may indicate that the SGMCs are dissipating their turbulent kinetic energy at different rates. The compact source could represent a short (~ 1 Myr) evolutionary stage in the early formation of super-star clusters.